# Difference between revisions of "UCSD-2019: Cross-Cut: Simulations for Measurement Requirements"

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* MHD: Dust + Synch small patches | * MHD: Dust + Synch small patches | ||

* d7 - implement in PySM 3 and increase resolution | * d7 - implement in PySM 3 and increase resolution | ||

− | * Currently used model up until DSR by the r-forecasting group: ** 00 - Simple Gaussian Sync/Dust with uniform amplitude across the sky ** 01 - PySM base (@zonca has higher nside than 512, to 4096? will get to 8192) ** 02 - PySM extended (@zonca has higher nside than 512, to 4096? will get to 8192) ** 03 - Same as 02 but Hensley/Draine dust model ** 04 - HiDPol dust model (by Tuhin Ghosh) ** 05 - Strong decorrelation model ** 06 - MHD based model from Flauger/Hensley (should swap in "08": one with more correct synchrotron) ** 07 - Amplitude modulated Gaussian ** 08 - MKD multilayer model from arxiv/1706.04162 ** 09 - Vansyngel model as described in arxiv/1611.02577 with multi-frequency extension | + | * Currently used model up until DSR by the r-forecasting group: |

+ | ** 00 - Simple Gaussian Sync/Dust with uniform amplitude across the sky | ||

+ | ** 01 - PySM base (@zonca has higher nside than 512, to 4096? will get to 8192) | ||

+ | ** 02 - PySM extended (@zonca has higher nside than 512, to 4096? will get to 8192) | ||

+ | ** 03 - Same as 02 but Hensley/Draine dust model | ||

+ | ** 04 - HiDPol dust model (by Tuhin Ghosh) | ||

+ | ** 05 - Strong decorrelation model | ||

+ | ** 06 - MHD based model from Flauger/Hensley (should swap in "08": one with more correct synchrotron) | ||

+ | ** 07 - Amplitude modulated Gaussian | ||

+ | ** 08 - MKD multilayer model from arxiv/1706.04162 | ||

+ | ** 09 - Vansyngel model as described in arxiv/1611.02577 with multi-frequency extension | ||

* For delensing, we need small scale polarized non-Gaussian Galactic foregrounds. Currently, only 09 has small scale NG. | * For delensing, we need small scale polarized non-Gaussian Galactic foregrounds. Currently, only 09 has small scale NG. | ||

* discuss: 00 should be replaced with 07? 00 won't be meaningfully used by the large area survey. But it is useful for the deep survey for sanity checks. | * discuss: 00 should be replaced with 07? 00 won't be meaningfully used by the large area survey. But it is useful for the deep survey for sanity checks. | ||

Line 91: | Line 101: | ||

==== Noise simulations for PWG ==== | ==== Noise simulations for PWG ==== | ||

− | * SAT | + | * SAT: start from BK data, fit noise model, just scaling NET and observing time, only data from Pole |

− | * BK | + | * BK NET calculator does not agree with data (in absolute terms), but only relative scaling matters |

* Noise calculator is just used for LAT | * Noise calculator is just used for LAT | ||

− | * Extrapolating 220 to 270, | + | * SAT: Extrapolating 220 to 270, 95GHz to lower freqs. Will need to be checked when data is available. |

* Check POLARBEAR new released performance, use that to scale? | * Check POLARBEAR new released performance, use that to scale? | ||

Delensing '''LAT''' at Pole needs a noise model, maybe scaling SPT?? | Delensing '''LAT''' at Pole needs a noise model, maybe scaling SPT?? |

## Latest revision as of 13:14, 19 October 2019

## Contents

## Charge

- How do we coordinate the production of a unified sky model with enough realism and flexibility for the AWGs?
- What simulations do we need for clusters and what cross-checks will be available with data?

## Agenda

Please add your name below the agenda if you plan to participate in the session, contact User:Zonca

- 5 min - Andrea Zonca: PySM 3, simulation tools developed for Simons Observatory
- 5 min - Marcelo Alvarez: Extragalactic modeling integration in PySM 3, Simulations requirements for cluster finding File:Exgal sims.pdf
- 5 min - Reijo Keskitalo: Scanning strategy for S4 Chile deep Chile wide Pole deep Pole wide
- 5 min - Ben Racine: Noise simulations for PGW analysis Sims for PGW
- 30 min - Discussion:
- Unified sky model
- How to gather requirements from AWG
- Clusters
- Plans for map-based simulations

Other participants: Raphael Flauger, Kimmy Wu

## Remote attendance

## Notes

Collaborative note taking on hackMD

# Cross-Cut: Simulations for Measurement Requirements

## Agenda and notes

- 5 min - Andrea Zonca: PySM 3, simulation tools developed for Simons Observatory
- 5 min - Marcelo Alvarez: Extragalactic modeling integration in PySM 3, Simulations requirements for cluster finding
- 5 min - Reijo Keskitalo: Scanning strategy for S4
- 5 min - Ben Racine: Noise simulations for PGW analysis
- 25 min - Discussion:

### Unified sky model

#### Galactic

- PySM (
`so_pysm_models`

) NSIDE 8192 Planck + Gaussian - MHD: Dust + Synch small patches
- d7 - implement in PySM 3 and increase resolution
- Currently used model up until DSR by the r-forecasting group:
- 00 - Simple Gaussian Sync/Dust with uniform amplitude across the sky
- 01 - PySM base (@zonca has higher nside than 512, to 4096? will get to 8192)
- 02 - PySM extended (@zonca has higher nside than 512, to 4096? will get to 8192)
- 03 - Same as 02 but Hensley/Draine dust model
- 04 - HiDPol dust model (by Tuhin Ghosh)
- 05 - Strong decorrelation model
- 06 - MHD based model from Flauger/Hensley (should swap in "08": one with more correct synchrotron)
- 07 - Amplitude modulated Gaussian
- 08 - MKD multilayer model from arxiv/1706.04162
- 09 - Vansyngel model as described in arxiv/1611.02577 with multi-frequency extension

- For delensing, we need small scale polarized non-Gaussian Galactic foregrounds. Currently, only 09 has small scale NG.
- discuss: 00 should be replaced with 07? 00 won't be meaningfully used by the large area survey. But it is useful for the deep survey for sanity checks.
- To generalize 08 and 09 into PySM, @zonca has to ask the creator of these models for code/info.
- Q: are there other Galactic models used in S4 outside of the r-forecasting group?
- Check consistency with Planck
- CO lines?

### How to gather requirements from AWG

### Extragalactic + Clusters

- Websky, 1 realization
- validated against planck
- lensing: 1 realization
- radio galaxy sources, catalog input, PySM component could generate map on the fly
- tSZ from Planck, CIB from Herschel and Planck, dusty galaxy count compared to Herschel, stack clusters

### Noise

#### Scanning strategy

- https://cmb-s4.org/wiki/index.php/Deeper_SAT_from_Chile_II
- https://cmb-s4.org/wiki/index.php/High_cadence_LAT_from_Chile

High cadence LAT gives lot of f_sky and daily scans for transients

Below only done in case of r detection from Deep SAT:

Jan & Feb we could remove

Clem has already noise pipeline

Delensing LAT from Pole??

#### Noise simulations for PWG

- SAT: start from BK data, fit noise model, just scaling NET and observing time, only data from Pole
- BK NET calculator does not agree with data (in absolute terms), but only relative scaling matters
- Noise calculator is just used for LAT
- SAT: Extrapolating 220 to 270, 95GHz to lower freqs. Will need to be checked when data is available.
- Check POLARBEAR new released performance, use that to scale?

Delensing **LAT** at Pole needs a noise model, maybe scaling SPT??